Correction to “Ionospheric convection response to slow, strong variations in a northward interplanetary magnetic field: A case study for January 14, 1988”

1994 ◽  
Vol 99 (A4) ◽  
pp. 6541 ◽  
Author(s):  
D. J. Knipp ◽  
B. A. Emery ◽  
A. D. Richmond ◽  
N. U. Crooker ◽  
M. R. Hairston ◽  
...  
Keyword(s):  
Magnetic Field ◽  
Interplanetary Magnetic Field ◽  
Ionospheric Convection

scholarly journals Ionospheric convection response to slow, strong variations in a northward interplanetary magnetic field: A case study for January 14, 1988

1993 ◽  
Vol 98 (A11) ◽  
pp. 19273-19292 ◽  
Author(s):  
D. J. Knipp ◽  
B. A. Emery ◽  
A. D. Richmond ◽  
N. U. Crooker ◽  
M. R. Hairston ◽  
...  
Keyword(s):  
Magnetic Field ◽  
Interplanetary Magnetic Field ◽  
Ionospheric Convection

Highly structured ionospheric convection for northward interplanetary magnetic field: A case study with DE 2 observations

1995 ◽  
Vol 100 (A8) ◽  
pp. 14743 ◽  
Author(s):  
S. Taguchi ◽  
M. Sugiura ◽  
T. Iyemori ◽  
J. D. Winningham ◽  
J. A. Slavin
Keyword(s):  
Magnetic Field ◽  
Interplanetary Magnetic Field ◽  
Ionospheric Convection

scholarly journals Dayside ionospheric response to changes in IMF polarity: optical and plasma-flow observations

2000 ◽  
Vol 18 (7) ◽  
pp. 782-788 ◽  
Author(s):  
S. E. Pryse ◽  
A. M. Smith ◽  
L. Kersley
Keyword(s):  
Magnetic Field ◽  
Interplanetary Magnetic Field ◽  
Plasma Flow ◽  
Line Emission ◽  
Line Of Sight ◽  
Magnetospheric Physics ◽  
Polar Cap ◽  
Ionospheric Response ◽  
Present Case Study

Abstract. The response of the dayside ionosphere to changes in polarity of the interplanetary magnetic field was observed by two independent techniques. The signatures were seen in the 630.0 nm red-line emission, measured by a meridian scanning photometer at Ny-Ålesund on Svalbard, and also in the line-of-sight plasma velocities monitored by the Finland CUTLASS SuperDARN radar. A time difference of some 6 to 8 min occurred between the responses of the two techniques, with the flows being first to respond. In the present case study, the longer delay in the optics suggests that ion precipitation controls the auroral emission.Key words: Ionosphere (ionosphere-magnetosphere interactions) · Magnetospheric physics (magnetosphere-ionosphere interactions; polar cap phenomena)

scholarly journals Different responses of northern and southern high latitude ionospheric convection to IMF rotations: a case study based on SuperDARN observations

2009 ◽  
Vol 27 (6) ◽  
pp. 2423-2438 ◽  
Author(s):  
D. Ambrosino ◽  
E. Amata ◽  
M. F. Marcucci ◽  
I. Coco ◽  
W. Bristow ◽  
...  
Keyword(s):  
Magnetic Field ◽  
High Latitude ◽  
Ionospheric Convection ◽  
Cell Pair ◽  
Cell Pattern ◽  
Southern High Latitude ◽  
Lobe Reconnection ◽  
Magnetospheric Field ◽  
The Imf

Abstract. We use SuperDARN data to study high-latitude ionospheric convection over a three hour period (starting at 22:00 UT on 2 January 2003), during which the Interplanetary Magnetic Field (IMF) flipped between two states, one with By>>|Bz| and one with Bz>0, both with negative Bx. We find, as expected from previous works, that day side ionospheric convection is controlled by the IMF in both hemispheres. For strongly northward IMF, we observed signatures of two reverse cells, both in the Northern Hemisphere (NH) and in the Southern Hemisphere (SH), due to lobe reconnection. On one occasion, we also observed in the NH two viscous cells at the sides of the reverse cell pair. For duskward IMF, we observed in the NH a large dusk clockwise cell, accompanied by a smaller dawn cell, and the signature of a corresponding pattern in the SH. On two occasions, a three cell pattern, composed of a large clockwise cell and two viscous cells, was observed in the NH. As regards the timings of the NH and SH convection reconfigurations, we find that the convection reconfiguration from a positive Bz dominated to a positive By dominated pattern occurred almost simultaneously (i.e. within a few minutes) in the two hemispheres. On the contrary, the reconfiguration from a By dominated to a northward IMF pattern started in the NH 8–13 min earlier than in the SH. We suggest that part of such a delay can be due to the following mechanism: as IMF Bx<0, the northward-tailward magnetosheath magnetic field reconnects with the magnetospheric field first tailward of the northern cusp and later on tailward of the southern cusp, due to the IMF draping around the magnetopause.

scholarly journals Response of ionospheric convection to changes in the interplanetary magnetic field: Lessons from a MHD simulation

2001 ◽  
Vol 106 (A10) ◽  
pp. 21429-21451 ◽  
Author(s):  
N. C. Maynard ◽  
G. L. Siscoe ◽  
B. U. Ö. Sonnerup ◽  
W. W. White ◽  
K. D. Siebert ◽  
...  
Keyword(s):  
Magnetic Field ◽  
Interplanetary Magnetic Field ◽  
Mhd Simulation ◽  
Ionospheric Convection
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